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It is often assumed that the "Kepler dichotomy" -- the apparent excess ofplanetary systems with a single detected transiting planet in the Keplercatalog -- reflects an intrinsic bimodality in the mutual inclinations ofplanetary orbits. After conducting 600 simulations of planet formation followedby simulated Kepler observations, we instead propose that the apparentdichotomy reflects a divergence in the amount of migration and the separationof planetary semimajor axes into distinct "clusters". We find that oursimulated high-mass systems migrate rapidly, bringing more planets into orbitalperiods of less than 200 days. The outer planets are often caught in amigration trap -- a range of planet masses and locations in which a dominantco-rotation torque prevents inward migration -- which splits the system intotwo clusters. If clusters are sufficiently separated, the inner cluster remainsdynamically cold, leading to low mutual inclinations and a higher probabilityof detecting multiple transiting planets. Conversely, our simulated low-masssystems typically bring fewer planets inside 200 days, forming a single clusterthat quickly becomes dynamically unstable, leading to collisions and highmutual inclinations. We propose an alternative explanation for the apparentKepler dichotomy in which migration traps during formation lead to fewerplanets inside the Kepler detection window, and where mutual inclinations playonly a secondary role. If our scenario is correct, then Kepler's STIPs (Systemswith Tightly-packed Inner Planets) are a sample of planets that escaped captureby co-rotation traps, and their sizes may be a valuable probe into thestructure of protoplanetary discs.

Migration traps as the root cause of the Kepler dichotomy